Principal-Axis Analysis of the Eddington Tensor for the Early Post-Bounce Phase of Rotational Core-Collapse Supernovae
arXiv:2109.05846 · doi:10.3847/1538-4357/ac714b
Abstract
Using full Boltzmann neutrino transport, we performed two-dimensional (2D) core-collapse supernova simulations in axisymmetry for two progenitor models with 11.2M and 15.0M both rotational and non-rotational. We employed the results obtained in the early post-bounce phase (t < 20 ms) to assess performance under rapid rotation of some closure relations commonly employed in the truncated moment method. We first made a comparison in 1D under spherical symmetry, though, of the Eddington factor p defined in the fluid rest frame (FR). We confirmed that the maximum entropy closure for the Fermionic distribution (MEFD) performs better than others near the proto-neutron star surface, where p < 1/3 occurs, but does not work well even in 1D when the phase space occupancy satisfies e < 0.5 together with p < 1/3, the condition known to be not represented by MEFD. For the 2D models with the rapid rotation, we employed the principal-axis analysis of the Eddington tensor. We paid particular attention to the direction of the longest principal axis. We observed in FR that it is aligned neither with the radial direction nor with the neutrino flux in 2D, particularly so in convective and/or rapidly rotating regions, the fact not accommodated in the moment method. We repeated the same analysis in the laboratory frame (LB) and found again that the direction of the longest principal axis is not well reproduced by MEFD because the interpolation between the optically thick and thin limits is not very accurate in this frame.
arXiv comment28pages, 22figures, accepted for publication in the ApJ
References in corpus (23)
- Physics of Core-Collapse Supernovae in Three Dimensions: a Sneak Preview
- Core-Collapse Supernova Explosion Theory
- Exploring Fundamentally Three-dimensional Phenomena in High-fidelity Simulations of Core-collapse Supernovae
- An Open-Source Neutrino Radiation Hydrodynamics Code for Core-Collapse Supernovae
- The Status of Multi-Dimensional Core-Collapse Supernova Models
- 2D Multi-Angle, Multi-Group Neutrino Radiation-Hydrodynamic Simulations of Postbounce Supernova Cores
- A Successful 3D Core-Collapse Supernova Explosion Model
- Fornax: a Flexible Code for Multiphysics Astrophysical Simulations
- A new multidimensional, energy-dependent two-moment transport code for neutrino-hydrodynamics
- Three-dimensional core-collapse supernova simulations of massive and rotating progenitors
- Neutrino Transfer in Three Dimensions for Core-Collapse Supernovae. I. Static Configurations
- Three-dimensional Boltzmann-Hydro code for core-collapse in massive stars I. special relativistic treatments
- Simulations of core-collapse supernovae in spatial axisymmetry with full Boltzmann neutrino transport
- A systematic study of proto-neutron star convection in three-dimensional core-collapse supernova simulations
- Three-Dimensional Core-Collapse Supernova Simulations with Multi-Dimensional Neutrino Transport Compared to the Ray-by-Ray-plus Approximation
- A new equation of state for core-collapse supernovae based on realistic nuclear forces and including a full nuclear ensemble
- A Detailed Comparison of Multi-Dimensional Boltzmann Neutrino Transport Methods in Core-Collapse Supernovae
- Three-dimensional Boltzmann-Hydro code for core-collapse in massive stars II. The Implementation of moving-mesh for neutron star kicks
- Analytic Closures for M1 Neutrino Transport
- On the Neutrino Distributions in Phase Space for the Rotating Core-collapse Supernova Simulated with a Boltzmann-neutrino-radiation-hydrodynamics Code
- Simulations of the Early Post-Bounce Phase of Core-Collapse Supernovae in Three-Dimensional Space with Full Boltzmann Neutrino Transport
- Three-Dimensional Boltzmann-Hydro Code for core-collapse in massive stars III. A New method for momentum feedback from neutrino to matter
- The Boltzmann-radiation-hydrodynamics Simulations of Core-collapse Supernovae with Different Equations of State: the Role of Nuclear Composition and the Behavior of Neutrinos